Ling-Jun Wang

The Most Luminous Supernova ASASSN-15lh: Signature of a Newborn Rapidly-Rotating Strange Quark Star

In this paper we show that the most luminous supernova discovered very recently, ASASSN-15lh, could have been powered by a newborn ultra-strongly-magnetized pulsar, which initially rotates near the Kepler limit. We find that if this pulsar is a neutron star, its rotational energy could be quickly lost as a result of gravitational-radiation-driven r-mode instability; if it is a strange quark star, however, this instability is highly suppressed due to a large bulk viscosity associated with the nonleptonic weak interaction among quarks and thus most of its rotational energy could be extracted to drive ASASSN-15lh. Therefore, we conclude that such an ultra-energetic supernova provides a possible signature for the birth of a strange quark star.

Superluminous Supernovae Powered by Magnetars: Late-time Light Curves and Hard Emission Leakage

Recently, researches performed by two groups have revealed that the magnetar spin-down energy injection model with full energy trapping can explain the early-time light curves of SN 2010gx, SN 2013dg, LSQ12dlf, SSS120810 and CSS121015, but fails to fit the late-time light curves of these Superluminous Supernovae (SLSNe). These results imply that the original magnetar-powered model is challenged in explaining these SLSNe. Our paper aims to simultaneously explain both the early- and late-time data/upper limits by considering the leakage of hard emissions. We incorporate quantitatively the leakage effect into the original magnetar-powered model and derive a new semi-analytical equation. Comparing the light curves reproduced by our revised magnetar-powered model to the observed data and/or upper limits of these five SLSNe, we found that the late-time light curves reproduced by our semi-analytical equation are in good agreement with the late-time observed data and/or upper limits of SN 2010gx, CSS121015, SN 2013dg and LSQ12dlf and the late-time excess of SSS120810, indicating that the magnetar-powered model might be responsible for these SLSNe and that the gamma ray and X-ray leakage are unavoidable when the hard photons were down-Comptonized to softer photons. To determine the details of the leakage effect and unveil the nature of SLSNe, more high quality bolometric light curves and spectra of SLSNe are required.

A Unified Energy-Reservoir Model Containing Contributions from 56 Ni and Neutron Stars and Its Implication to Luminous Type Ic Supernovae

Most type-Ic core-collapse supernovae (CCSNe) produce

A Triple-Energy-Source Model for Superluminous Supernova iPTF13ehe

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PTF11agg AS THE FIRST EVIDENCE FOR REVERSE SHOCK EMISSION FROM A POST-MERGER MILLISECOND MAGNETAR

Ni and neutron stars (NSs) or black holes (BHs). The dipole radiation of nascent NSs has usually been neglected in explaining supernovae (SNe) with peak absolute magnitude

Optical Transients Powered by Magnetars: Dynamics, Light Curves, and Transition to the Nebular Phase

M_{\rm peak}

PROBING THE BIRTH OF POST-MERGER MILLISECOND MAGNETARS WITH X-RAY AND GAMMA-RAY EMISSION

in any band are

REVERSE SHOCK EMISSION AND IONIZATION BREAKOUT POWERED BY POST-MERGER MILLISECOND MAGNETARS

\gtrsim -19.5

A Monte Carlo Approach to Magnetar-powered Transients: I. Hydrogen-deficient Superluminous Supernovae

~mag, while the

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

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